Notes. (1) Source name; (2) average column density (N_H, Z = N_H, S90 = N_H, S0) in units of 10²⁴ cm⁻²; (3) coronal temperature (keV); values with no error bar were unconstrained and have been fixed to a value of 50 keV. (4) optical depth; values with no error bars were unconstrained and have been fixed to a value of τ = 2. (5) the high energy cut-off derived by Ricci et al. (2017) from Neil Gehrels Swift, XMM-Newton, Chandra joint fits; and (6) unobscured reflected fraction in the 20–40 keV band. The unobscured reflection fraction is defined as Flux[S0]/(Flux[Z]+Flux[S90]+Flux[S0]); (8) χ² over degrees of freedom. (9) References for previous NuSTAR analyses. References. (a) Bauer et al. (2015); (b) Arévalo et al. (2014) ; (c) Puccetti et al. (2014); (d) Puccetti et al. (2016); (e) Baloković et al. (2014); (f) Masini et al. (2016) (g) Koss et al. (2015) (h) Annuar et al. (2015) (i) Marchesi et al. (2018).